Understanding Submillimetre Galaxies: Lessons from Low Redshifts

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1 #SMG20 Durham 2017 Understanding Submillimetre Galaxies: Lessons from Low Redshifts Paul van der Werf Leiden: Marissa Rosenberg Rowin Meijerink Saskia van den Broek Edo Loenen Kirsty Butler Cardiff/ESO:Padelis Papadopoulos ESTEC: Kate Isaak Groningen: Marco Spaans Madrid: Santiago Garcia-Burillo MPIfR: Axel Weiß UCL: Thomas Greve

2 Know your classics Casey, Narayanan, & Cooray 2014, Phys Rep, 541, 45 Carilli & Walter 2013, ARA&A, 51, 105 Blain, Smail, Ivison, Kneib & Frayer, 2002, Phys Rep, 369, 111 Scoville, 2012, Canary Winter School, arxiv/

3 Outline ULIRGs vs. SMGs Local physical conditions from FIR-submm spectra Molecular gas mass Gas outflows

4 From IRTRONs to ULIRGs : IRAS ( ultra-high luminosity : Houck et al., 1985)

5 Local ULIRGs are major mergers (GOALS - Evans et al.) At L IR > L ʘ, all (U)LIRGs show merging signatures

6 Babies or monsters? Cool ULIRG Warm ULIRG QSO (Sanders et al., 1988)

7 Extreme star formation L IR /L CO SFR/M H 2 SFE ULIRGs : L M FIR H L M 1 (Gao & Solomon, 2001) Milky Way : Galactic GMCs : OMC -1: Orion BN - KL : 1.5 L 1.8 L 54 L 400 L M M M M 1 L IR SFR

8 Strong evolution (Casey et al., 2014)

9 ULIRGs vs. SMGs Where does the analogy break down? At same L IR, T d is lower at high z CO disks in SMGs are larger than in ULIRGs Position with respect to Galaxy Main Sequence? (Casey et al., 2014)

10 ULIRGs vs. SMGs CO ladders NB: selection, diversity (Greve et al., 2014)

11 Outline ULIRGs vs. SMGs Local physical conditions from FIR-submm spectra Molecular gas mass Gas outflows

12 Mrk 231 Herschel SPIRE FTS (Van der Werf et al., 2010)

13 Mrk 231 CO ladder 2 PDRs + XDR 6.4:1:4.0 n=10 4.2, F X =28 * n=10 3.5, G 0 = n=10 5.0, G 0 = (Van der Werf et al., 2010) * 28 erg cm -2 s -1 G 0 =10 4.2

14 XDRs vs. PDRs Physical differences X-rays penetrate much larger column densities than UV photons Gas heating efficiency in XDRs is 10 50%, compared to <1% in PDRs Dust heating much more efficient in PDRs than in XDRs CO/[CII] elevated in XDRs compared to PDRs

15 XDRs vs. PDRs CO ladder Identical total incident energy (Spaans & Meijerink, 2008)

16 PAH 6.2 EW traces starburst fraction CO cooling fraction as AGN tracer HerCULES sample Mrk231 IRASF (Rosenberg et al., 2015)

17 CO ladders of local (U)LIRGs Herschel SPIRE/FTS data from HerCULES Identical total incident energy α < < α < 0.66 α > 0.66 α = CO(12 11)+CO(13 12) CO(5 4)+CO(6 5) (Rosenberg et al., 2015)

18 Starburst and AGN tracers Principal component analysis of HerCULES lines starbursts CO excitation is the best AGN indicator AGNs ([CII]+[OI])/FIR high in starbursts OH + and H 2 O + do not prefer AGNs (Van den Broek et al., in prep.)

19 MPDRs and CRDRs CO ladder For almost all starbursts, UV heating (PDR) is insufficient. MPDRs or CRDRs are needed. Extreme MPDRs are hard to distinguish from XDRs. (Kazandjian et al., 2015)

20 Fine-structure line deficits GOALS sample - [CII] 158μm, [NII] 122/204μm, [OI] 63μm, [OIII] 88μm (Casey et al., 2014) (Diaz-Santos et al., 2017) offset only due to larger size?

21 [CII] line deficit at for SMGs SPT sample (Spilker et al., 2016)

22 Line deficits and physical conditions PDR modeling based on [CII], [OI] and [NII] Transition in properties at IR = L ʘ /kpc 2 (Diaz-Santos et al., 2017)

23 Outline ULIRGs vs. SMGs Local physical conditions from FIR-submm spectra Molecular gas mass Gas outflows

24 H 2 mass from observations of other tracers the invisible molecule H 2 observe excitation of other species = observe H 2 through its collisions Modeling excitation yields conversion factor to H 2 mass

25 Star formation laws and α CO (Casey et al., 2014)

26 α CO from improved data and modeling See talk by Weiß Weiß et al., in prep.

27 Outline ULIRGs vs. SMGs Local physical conditions from FIR-submm spectra Molecular gas mass Gas outflows

28 Self-regulated galaxy buildup Theoretical paradigm gas inflow star forming gas feedback gas outflow extremely difficult to observe observable Infrared, Hα, CO, HCN, dust, etc observable Supernova remnants, AGNs observable CO, Hα, X-rays, etc.

29 Mrk 231 outflow in CO (Feruglio et al., 2010) H 2 O absorption H 2 O emission

30 Mrk 231 outflow in CO and HCN (Aalto et al., 2014) The outflowing molecular gas is dense!

31 Multi-phase outflows CO ladder Complex structure and velocity field Out-of-equilibrium chemistry Relative and total masses? Observations of multiple phases needed (Wada, Schartmann, & Meijerink, 2016)

32 Hα supernebulae around (U)LIRGs NGC6240 R Hα (Armus et al., 1990)

33 Ubiquity of molecular outflows Do galaxies where the integrated spectrum does not show wings have no outflows? NGC1068, ALMA (García-Burillo et al., 2014)

34 NGC1068 velocity field

35 NGC1068 outflow

36 IRAS

37 IRAS outflow (García-Burillo et al., 2015)

38 Driving (García-Burillo et al., 2015)

39 Outflow tracers Can we use OH + and CO(9 8) to trace high-z outflows?

40 OH + outflow at z = 2.41

41 OH + in Arp220 Herschel/SPIRE, Rangwala et al., 2012

42 Hot off the press: OH + in Arp220 with ALMA Band 10 NH 2 OH+ red wing OH + blue wing OH + main absorption

43 Open questions CO ladder: what is the role of mechanical and cosmic ray heating and what can we learn from it? Fine-structure lines: are there deviations from the low-z relation? What happens at low metallicities? Outflows: how do outflow properties depend on galaxy properties? What is the mass outflow rate? What happens to the outflowing gas? Extreme star formation: Is Eddington-limited star formation really relevant? Arp220: What is happening in the obscured nuclei? How can we tell? SMGs vs. ULIRGs: what do the differences mean? IMF: universal? Top-heavy? How can we tell?

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